Cosmic Ray-Modified Astrophysical Shocks: Modeling and Observations

宇宙射线修正的天体物理冲击：建模和观测

• 批准号: 1306672
• 负责人: Maxim Lyutikov
• 金额: $ 40.57万
• 依托单位: Purdue University
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2013
• 资助国家: 美国
• 起止时间: 2013-09-01 至 2018-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1306672&HistoricalAwards=false
• 关键词: Cosmic; Ray; Modified; Astrophysical; Shocks

The current dominant paradigm in cosmic ray (CR) research says that the bulk of Galactic CRs with energies below a peta-electron volt are created in supernova remnants (SNRs) via diffusive shock acceleration. This is now at a turning point: soon, the comparison between theoretical calculations and observations from the radio band to gamma rays to high energy neutrinos is expected to either confirm the paradigm or call for a paradigm shift. This project will develop novel theoretical and observational techniques to test the SNR paradigm. The theoretical studies are based around a common theme: how do cosmic rays modify the structure of the shock? The work will investigate magnetic field amplification, injection and acceleration of CRs, and the role of dust sputtering and the large neutral component in the upstream plasma. Analysis of neutral hydrogen in the so-called Balmer-dominated shocks should lead to a novel way to measure the shock acceleration efficiency. The research will include consideration of how cosmic rays escape their acceleration sites and propagate towards the Earth and of the kinetic diffusion of CRs. Modeling of time- and spatially-dependent particle dynamics will be compared with observed non-thermal filaments and tied to the results of high energy particle observations.This is a multidisciplinary project involving data analysis and theoretical and computational work in astrophysics and plasma physics. Work with students in the Purdue Computer Graphics Technology Department will lead to an interactive kiosk, in partnership with Purdue's Discovery Learning Center, to explain about CRs to all visiting groups, including K-12 students, teachers, and the general public.

宇宙射线（CR）研究中的当前主要范式表明，在PETA-电子伏特以下的能量的大部分CR是通过扩散的冲击加速器在超新星残留物（SNRS）中产生的。 现在是一个转折点：很快，预计从无线电频段到伽马射线到高能量中微子的理论计算与观察结果之间的比较有望确认范式或要求进行范式移动。 该项目将开发出新颖的理论和观察技术来测试SNR范式。 理论研究基于一个共同的主题：宇宙射线如何修改冲击的结构？ 这项工作将研究CRS的磁场扩增，注入和加速度，以及灰尘溅射和上游血浆中大型中性成分的作用。 在所谓的Balmer主导的电击中对中性氢的分析应导致一种新颖的方法来测量冲击加速度的效率。 该研究将包括考虑宇宙射线如何逃脱其加速位点并向地球传播和CRS动力学扩散。 时间和空间依赖性粒子动力学的建模将与观察到的非热丝进行比较，并与高能量粒子观察结果相关联。这是一个涉及数据分析以及天体物理学和质量物理学的理论和计算工作的多学科项目。 与普渡大学图形技术系的学生合作将与普渡大学的发现学习中心合作，向所有访问团体（包括K-12学生，老师和公众）解释CRS。